adsabs/AstroCLIMB huggingface dataset:
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Cumulative distributions of the detection efficiency, for the S/Ns and for the error on the parameters, for BBH signals with the three considered network configuration, using the waveform model IMRPhenomHM.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Histograms of the S/N and parameter errors for BBHs for ET alone, using the waveform model IMRPhenomHM, which includes subdominant modes of the signal, and IMRPhenomD, which only contains the quadrupole. For the S/N, in each bin, we show the fraction of events, normalized to the total number of sources in our sample. For the parameters of the waveform, we limit to the ﹩{\tilde{N}}_{\det }﹩ events that pass the cut S/N ≥ 12, and that furthermore admit a reliable inversion of the Fisher matrix, and we show the fraction of events, normalized to ﹩{\tilde{N}}_{\det }﹩.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: As in Figure 6, for the ET+2CE network. We here further show the results obtained without imposing the 85% uncorrelated duty cycle for the detectors.
Paper: Mapping Dark Matter with Extragalactic Stellar Streams: The Case of Centaurus A
Authors: Sarah Pearson, Adrian M. Price-Whelan, David W. Hogg, Anil C. Seth, David J. Sand, Jason A. S. Hunt, Denija Crnojević
Figure caption: Visualization of the best-fit model stream from Figure 4 with ﹩{v}_{{\phi }_{1}}﹩ = 460 km s−1 and ﹩{v}_{{\phi }_{2}}﹩ = 50 km s−1 and ﹩-\mathrm{ln}{ \mathcal L }=3.16﹩. Upper panels: The model stream transformed to ICRS coordinates, colored by radial velocity in Cen A’s rest frame (left) and distance along the stream with respect to Cen A (right), overplotted on the Cen A image data. The white arrow indicates the direction of motion of Dw3, and the black points are the 13 control data points, x  n  (see also orange points in Figure 1). Lower left: The best-fit model stream shown in (ϕ 1, ϕ 2) space in degrees (see Section 3.2). The orange points are the 13 control data points, x  n , the green points (colored by radial velocity) are the simulated model stream, the gray line is the center point of the simulated model stream, and the gray dots are the 13 simulated stream center points, y  n , at the ϕ 1 location of the control data. The black arrow indicates the direction of motion of Dw3. Lower right: The evolution of the 3D position in kpc of the progenitor with respect to Cen A’s center as a function of time (black line, t = 0 at present day). The vertical lines mark the pericenter passages of the progenitor.
Paper: Mapping Dark Matter with Extragalactic Stellar Streams: The Case of Centaurus A
Authors: Sarah Pearson, Adrian M. Price-Whelan, David W. Hogg, Anil C. Seth, David J. Sand, Jason A. S. Hunt, Denija Crnojević
Figure caption: Summary of ﹩-\mathrm{ln}{ \mathcal L }﹩ values (Equation (2); see color bar) for model streams initiated with a fixed radial velocity of v rad = −181.4 km s−1, but with various combinations of ﹩{v}_{{\phi }_{1}}﹩ and ﹩{v}_{{\phi }_{2}}﹩. The fits of each stream to the control data are evaluated as described in Section 3.2. The blank space represents the region of the orbit parameter space, where the simulated streams were disregarded because they were shorter than the extent of the control data. Note that the maximal color bar value is ﹩-\mathrm{ln}{ \mathcal L }﹩ = 50 for visualization purposes but some of the fits are extremely poor with ﹩-\mathrm{ln}{ \mathcal L }\gt 1000﹩. Left: A small pocket of orbits (﹩{v}_{{\phi }_{1}}\sim 300﹩–800 km s−1 and ﹩{v}_{{\phi }_{2}}\sim 40﹩–100 km s−1) that produce good fits to the data (see gray rectangle). Upper right: Zoomed version of gray rectangle in the left panel, where we resolve the combination of ﹩{v}_{{\phi }_{1}}﹩ and ﹩{v}_{{\phi }_{2}}﹩ that produced good fits to the data before any Jacobi criterion is applied. Lower right: Same as above, but after the Jacobi criterion has been applied. The model stream that produced the best fit has ﹩{v}_{{\phi }_{1}}﹩ = 460 km s−1 and ﹩{v}_{{\phi }_{2}}﹩ = 50 km s−1 with ﹩-\mathrm{ln}{ \mathcal L }=3.16﹩ in both cases.
Paper: Mapping Dark Matter with Extragalactic Stellar Streams: The Case of Centaurus A
Authors: Sarah Pearson, Adrian M. Price-Whelan, David W. Hogg, Anil C. Seth, David J. Sand, Jason A. S. Hunt, Denija Crnojević
Figure caption: Top: Enclosed mass of the fiducial potential as a function of galactic radius (black solid line). This potential includes a Hernquist stellar component and an NFW dark matter halo component (M 200,fiducial = 9.4 × 1012 M ⊙) motivated from GC kinematic estimates within 40 kpc (Woodley et al. 2010; see black data point). The colored lines show a range of potentials with the same Hernquist stellar component, but with varying NFW profiles (colored lines; M 200 = 0.94–17.86  × 1012 M ⊙, where red is Halo 1 and blue is Halo 10), which we use throughout the paper (see also Table 2). We use the halo mass vs. halo concentration relation from Muñoz-Cuartas et al. (2011). The vertical teal line shows the projected distance from Dw3 to the center of Cen A. Bottom: Circular velocity as a function of galactic radius for the fiducial potential (black line) as well as the range of potentials (colored lines).
Paper: Mapping Dark Matter with Extragalactic Stellar Streams: The Case of Centaurus A
Authors: Sarah Pearson, Adrian M. Price-Whelan, David W. Hogg, Anil C. Seth, David J. Sand, Jason A. S. Hunt, Denija Crnojević
Figure caption: The outer stellar halo density map of RGB stars from Crnojević et al. (2016) obtained with the Magellan Clay 6.5 m telescope calibrated to be in units of M ⊙pc−2. We have overplotted 13 control data stream center points (black) along the Dw3 Stream and three control points (white) along the second stream in Cen A. Note that the actual Cen A galaxy is very small compared to the stellar halo mapped here.
Paper: Mapping Dark Matter with Extragalactic Stellar Streams: The Case of Centaurus A
Authors: Sarah Pearson, Adrian M. Price-Whelan, David W. Hogg, Anil C. Seth, David J. Sand, Jason A. S. Hunt, Denija Crnojević
Figure caption: The same data as shown in Figure 1, but here we overplot the two other coordinate systems used in the paper: the galactic coordinate system (x, y, z) used for stream modeling (red), as well as the ϕ 1, ϕ 2 coordinate system that is centered on Cen A and rotated by 47.76 deg, such that Dw3 is located at ϕ 1 = 0 (white). We use the latter to visualize our mock stream fits throughout the paper.
Paper: The Merger Rate of Primordial Black Hole–Neutron Star Binaries in Ellipsoidal-collapse Dark Matter Halo Models
Authors: Saeed Fakhry, Zahra Salehnia, Azin Shirmohammadi, Javad T. Firouzjaee
Figure caption: Merger rate of PBH–NS binaries within each halo for ellipsoidal- and spherical-collapse halo models as a function of halo virial mass in the present-time universe. The shaded red band shows this relation for ellipsoidal-collapse halo models, while the shaded blue band indicates it for spherical-collapse halo models. The NFW density profile has been utilized.
Paper: Transition Energies and Line Oscillator Strengths of the C 2Π(0)-X 2Π(0–6) Absorption Bands of Nitric Oxide. A Theoretical Study
Authors: C. Lavín, A. M. Velasco
Figure caption: A comparative plot of the present f-values and those deduced from Einstein emission coefficients data of Qu et al. (2021a).
Paper: Transition Energies and Line Oscillator Strengths of the C 2Π(0)-X 2Π(0–6) Absorption Bands of Nitric Oxide. A Theoretical Study
Authors: C. Lavín, A. M. Velasco
Figure caption:  C 2Π-fraction of the C 2Π1/2 and C 2Π3/2 rotational levels of NO calculated from the state mixing model, as discussed in the text.
Paper: The Merger Rate of Primordial Black Hole–Neutron Star Binaries in Ellipsoidal-collapse Dark Matter Halo Models
Authors: Saeed Fakhry, Zahra Salehnia, Azin Shirmohammadi, Javad T. Firouzjaee
Figure caption: Total merger event rate of PBH–NS binaries for ellipsoidal-collapse dark matter halo models as a function of the upper bounds on the PBH fraction and their masses. The solid black, dashed red, and dotted–dashed blue lines indicate this relation while considering PBH mass to be M PBH = 5M ⊙, 20M ⊙, and 50M ⊙, respectively. The shaded band indicates the total merger rate of BH–NS binaries recorded by the LIGO–Virgo detectors, i.e., 7.8–140 Gpc−3 yr−1.
Paper: The Merger Rate of Primordial Black Hole–Neutron Star Binaries in Ellipsoidal-collapse Dark Matter Halo Models
Authors: Saeed Fakhry, Zahra Salehnia, Azin Shirmohammadi, Javad T. Firouzjaee
Figure caption: Merger rate of PBH–NS binaries per unit time and per unit volume for ellipsoidal- and spherical-collapse halo models as a function of halo virial mass in the present-time universe. The shaded red band shows this relation for ellipsoidal-collapse halo models, while the shaded blue band represents it for spherical-collapse halo models. The NFW density profile has been utilized.
Paper: The Merger Rate of Primordial Black Hole–Neutron Star Binaries in Ellipsoidal-collapse Dark Matter Halo Models
Authors: Saeed Fakhry, Zahra Salehnia, Azin Shirmohammadi, Javad T. Firouzjaee
Figure caption: Upper limit of the merger event rate of PBH–NS binaries for ellipsoidal-collapse dark matter halo models as a function of redshift. The solid red line represents this relation for the Einasto density profile, while the dashed black line shows it for the NFW density profile.
Paper: Detection of the Extended γ-Ray Emission from the High Galactic Latitude Calvera’s SNR Candidate
Authors: Yuliang Xin, Xiaolei Guo
Figure caption: Left: 2.°0 × 2.°0 TS map for photons above 1 GeV. The TS map is smoothed with a Gaussian kernel of σ = 0.°02. The white sold circle shows the best-fit radius of the uniform disk for the spatial template of SrcX. The black diamond reveals the Calvera pulsar PSR J1412+7922. And the cyan cross marks the fitting position of SrcX as a point source. Two green dashed circles describe the ring morphology of the diffuse radio emission (Calvera’s SNR) by LOFAR at 144 MHz (Arias et al. 2022). Right: SED of SrcX. The black arrows indicate the 95% upper limits and the gray histogram shows the TS value for each energy bin. The green solid and dashed lines show the best-fit power-law spectrum and its 1σ statistic error in the energy range of 100 MeV–1 TeV. The red sold line is the best-fit log-parabola spectrum.
Paper: Detection of the Extended γ-Ray Emission from the High Galactic Latitude Calvera’s SNR Candidate
Authors: Yuliang Xin, Xiaolei Guo
Figure caption: Modeling of the multiwavelength SED of Calvera’s SNR. The left panel is for the leptonic model, where the power-law spectra with indices of 2.0 and 2.4 for electrons are presented by the black solid and gray dashed lines, respectively. The radio emission is dominated by the synchrotron component, shown as the  green dashed curve. For γ-ray emission, the contribution of the ICS emission includes three components from the CMB (blue dashed), infrared (magenta dashed), and optical (green dashed) radiation fields. The right panel is for the hadronic model, where the PL and BPL models are presented by the black solid and gray dashed lines, respectively. The contribution from the pion-decay process with the PL model is shown as the red dashed line. The flux of the bremsstrahlung component is too low to show, and the black solid line represents the sum of the different radiation components. The gray dotted–dashed line shows the differential sensitivity of CTA-North (50 hr; C. T. A. Consortium et al. 2019).
Paper: Quantum Chemical Computations of Gas-phase Glycolaldehyde Deuteration and Constraints on Its Formation Route
Authors: Fanny Vazart, Cecilia Ceccarelli, Nadia Balucani, Dimitrios Skouteris
Figure caption: Summary of the multistep reactions with their respective major products. Reactions are numbered as in Table 1. The colored boxes show the parent–daughter relationship. The magenta boxes show the channels that lead to undeuterated glycolaldehyde products (8b and 9b). Note that the two types of CH2DCH2OH (a-a and a-s) are characterized by different spectroscopic properties that make them observationally distinguishable. They are characterized, however, by very similar chemical behavior. Branching ratios are also indicated (see text).
Paper: Quantum Chemical Computations of Gas-phase Glycolaldehyde Deuteration and Constraints on Its Formation Route
Authors: Fanny Vazart, Cecilia Ceccarelli, Nadia Balucani, Dimitrios Skouteris
Figure caption: Genealogical tree of ethanol (adapted from Skouteris et al. 2018) The numbers in the figure indicate the branching ratios. The present study focuses only on the reactions leading to glycolaldehyde, shown in the red boxes.
Paper: Near-infrared Spectroscopy of a Massive Young Stellar Object in the Direction toward the Galactic Center: XCN and Aromatic C–D Features
Authors: Takashi Onaka, Itsuki Sakon, Takashi Shimonishi
Figure caption: Schematic view of the proposed geometry. The ice layer has a slab-like shape (gray slab), separated from the central ionized region. The ionized region has a compact ionizing source (red star in the brown region), which provides strong UV radiation, surrounded by an extended region (yellow region, Kim & Koo 2001). The intensity of the UV radiation on the surface of the ice layer (blue arrows) varies with the distance from the central source, affecting the efficiency of the formation of the XCN carriers. The width of the arrow schematically indicates the intensity of the UV radiation at the surface of ice layer. The light green region is a PDR, where PAH and deuterated PAH emission arise. The dashed arrow shows the light rays to the observer.
Paper: Near-infrared Spectroscopy of a Massive Young Stellar Object in the Direction toward the Galactic Center: XCN and Aromatic C–D Features
Authors: Takashi Onaka, Itsuki Sakon, Takashi Shimonishi
Figure caption: Correlations of the 4.4 μm excess emission with (a) the 3.3 μm emission, (b) H I Brα, (c) the H2O ice column density, and (d) the extinction at Brα. The intensities of the 4.4 and 3.3 μm emissions, and Brα are corrected for the foreground extinction.
Paper: Detection of the Extended γ-Ray Emission from the High Galactic Latitude Calvera’s SNR Candidate
Authors: Yuliang Xin, Xiaolei Guo
Figure caption: Typical γ-ray SEDs of several prominent SNRs. The energy fluxes of Calvera’s SNR are scaled upward by 40 times for comparison.
Paper: Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST
Authors: Francesco Iacovelli, Michele Mancarella, Stefano Foffa, Michele Maggiore
Figure caption: Redshift distributions of the BNSs observed at ET alone, selected on the basis of different thresholds for the S/N (left panel), or setting S/N ≥ 12 and applying further cuts on Δd  L /d  L  (central panel), or on ΔΩ90% (right panel). The black solid line corresponds to the total BNS population in the astrophysical model that we have assumed. We set ﹩{{ \mathcal R }}_{0,\mathrm{BNS}}=105.5\,{\mathrm{Gpc}}^{-3}\,{\mathrm{yr}}^{-1}﹩, and show the results for the detections in 1 yr (taking into account our assumptions of the duty cycle). Given the uncertainly on ﹩{{ \mathcal R }}_{0,\mathrm{BNS}}﹩, which currently can be in the range (10–1700) Gpc−3 yr−1, one should keep in mind that the absolute number can still change by a factor ﹩{ \mathcal O }\left(10\right)﹩ or more. In each column, the upper panel shows the number of events per redshift bin, while the lower panel shows the corresponding cumulative distributions, normalized to the number of BNS events in our sample, N BNS = 105.